The SWICS 2.0 dataset consists of time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic distribution of heavy ions in the solar wind. This data set begins after August 23, 2011, when a radiation and age-induced hardware anomaly altered the instrument's operational state. It should not be confused with SWICS 1.1, the recalibrated data set extending from launch up to the anomaly.
SWICS 2.0 continues to make heavy ion measurements which are not available from any other instrument, and new data analysis methods have been developed to address the statistical and calibration issues of the current instrument state.

The Solar Wind Ion Composition Spectrometer (SWICS) Solar Wind Data set consists of time series measurements of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. Time resolutions: 1 hour, 2 hour, and 1 day. (Not all products are delivered at all time-resolutions.)
This descriptor comprises two sets of data:
(1)The SWICS 1.1 data set which covers launch up to August 23, 2011, when a radiation and age-induced hardware anomaly altered the instrument's operational state.
(2)The SWICS 2.0 data set which begins after August 23, 2011, and includes a subset of the items included in the SWICS 1.1 data set, as well as the O+8/O+6 ratio.

This ACE SWICS 1.1 data set contains Solar Wind Ion Composition Spectrometer (SWICS) level-2 daily averaged solar wind parameters, including
composition (He/O, C/O, N/O, Ne/O, Mg/O, Si/O, S/O, Fe/O), bulk ion speed (He+2) and charge states (C+6/C+5, O+7/O+6 Carbon, Oxygen, Fe) at all solar wind speeds above 300 km/s (protons) and 170 km/s (Fe+16). Distribution functions of H and He isotopes are measured of both solar and interstellar sources up to energies of 100 keV/e. Please note the N/O and S/O composition data are not present in the 1-hour or 2-hour SWICS datasets. This SWICS 1.1 dataset consists of a re-release of significantly improved time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. It is a major new version produced with completely redesigned analysis methods to account more rigorously for instrumental and statistical effects (Shearer et al. 2014). Rare elements are now identified more reliably and estimates of statistical error are provided. These release notes describe the data, the methods used to determine them, and issues of data quality and measurement uncertainty.

This ACE SWICS 1.1 data set contains Solar Wind Ion Composition Spectrometer (SWICS) level-2 2-hr averaged solar wind parameters, including density (He+2), bulk and thermal ion speeds (He+2, C+5, O+6, Fe+10), composition (He/O, C/O, Ne/O, Mg/O, Si/O, Fe/O), and charge states (C+6/C+5, O+7/O+6 Carbon, Oxygen, Fe, Ne, Mg, Si) and solar wind type indicators at all solar wind speeds above 300 km/s (protons) and 170 km/s (Fe+16). Distribution functions of H and He isotopes are measured of both solar and interstellar sources up to energies of 100 keV/e. This SWICS 1.1 dataset consists of a re-release of significantly improved time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. It is a major new version produced with completely redesigned analysis methods to account more rigorously for instrumental and statistical effects (Shearer et al. 2014). Rare elements are now identified more reliably and estimates of statistical error are provided. These release notes describe the data, the methods used to determine them, and issues of data quality and measurement uncertainty.

This ACE SWICS 1.1 data set contains Solar Wind Ion Composition Spectrometer (SWICS) level-2 2-hr data of actual Q-state distributions of carbon, oxygen, neon, magnesium, silicon and iron, as opposed to the averaged Q-states that have been available on CDAWeb for some time. This SWICS 1.1 dataset consists of a re-release of significantly improved time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. It is a major new version produced with completely redesigned analysis methods to account more rigorously for instrumental and statistical effects (Shearer et al. 2014). Rare elements are now identified more reliably and estimates of statistical error are provided. These release notes describe the data, the methods used to determine them, and issues of data quality and measurement uncertainty.

ACE SWICS_SWIMS 1.1 L2 1-hr, 1-d, 27-d solar wind He, Mg, O, Fe TnV data, plus species ratios and charge states, at ASC. This SWICS 1.1 dataset consists of a re-release of significantly improved time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. It is a major new version produced with completely redesigned analysis methods to account more rigorously for instrumental and statistical effects (Shearer et al. 2014). Rare elements are now identified more reliably and estimates of statistical error are provided. These release notes describe the data, the methods used to determine them, and issues of data quality and measurement uncertainty.

These are daily, instrument-specific plots of data from all the AMPTE/CCE instruments. For the energetic particle data of the CHEM, HPCE and MEPA instruments, the data are spectrograms with color coded count rates or fluxes vs. time and vs. any one of several available independent variables. For the magnetic field and plasma wave data from MFE and PWE, the plots are simpler intensity-vs-time plots.

AMPTE/CCE CHEM data consist of rates and fluxes of ions H through Fe with energies between 3 and 300 keV/q, as functions of mass, mass/charge, energy, and
arrival direction. Time resolution in the Earth's magnetosphere and magntosheath is less than 1 minute. Data were originally in VMS binary. Data are now in daily gzipped FITS files as translated from the original VMS binaries.

These data consist of plots of color-coded ion
count rates vs. spin phase angle and time, for thermal H+, He++,
He+ and O+ ions and for suprathermal H+ and O+ ions. Each plot
covers some or all of one ~3.5 hour orbit. Digital binary data
and a data reading program are also accessible.

These count rate data reside in the DARTS/Akebono
binary Science DataBase (SDB). They consist of count rates at 8-sec
spacecraft spin resolution, separately for thermal and suprathermal
H+, He+ and O+ ions. Detailed information and a data-read program
are found at http://darts.isas.jaxa.jp/akbn/readme/readme.sms.txt.

The Cluster Ion Spectrometry (CIS) data products include three-dimensional ion distributions (about 0-40 keV/e) in 4-s spacecraft spin resolution and mass-per-charge composition distribution that are measured by the Hot Ion Analyzer (HIA) and Composition Distribution Function (CODIF) analyzer on board the Cluster II Rumba spacecraft. Data products consist of processed raw data (Level 1 data), moments of the distribution functions (Level 2 data), and calibrated high-resolution data in a variety of physical units (Level 3 data). Furthermore, the calibration files and high-level processing software are also available.
CIS Level 1 data are decommutated, decompressed and time-tagged telemetry data in raw instrument units.
CIS Level 2 data are moments of the particle functions: ion density, velocity in the GSE reference frame, and temperature in parallel and perpendicular components (obtained by diagnolizing the pressure tensor). For CODIF, which has a higher upper energy limit than HIA, the pressure is also supplied in addition. They correspond to the Prime Parameters from the Cluster Science Data System: onboard calculated moments, then reprocessed on ground (total efficiency calibration adjustments, coordinate transformations etc.). Onboard calculated moments provide 1-spin time resolution, and are calculated from the full angular and energy resolution 3-D ion distributions.
In addition to the onboard calculated moments, CIS Level 2 data include also CODIF moments calculated on the ground from the 3-D ion distributions. These provide better calibration adjustments (per anode efficiency) and are thus more accurate, but have a reduced time and energy resolution. HIA on the ground calculated moments are not supplied, because the same anode calibrations would be used as for the onboard calculated ones, but with a degraded time, energy and angular resolution (no added value). A software package is available for download at the CAA web site, allowing the user to interactively calculate partial (or total) moments of the ion distributions, for selected energy and solid angle ranges: CODIF (all 4 ion species) and HIA data.
CIS Level 3 data are processed high-resolution 3-D ion distributions. They are produced by correcting the Level 1 data for detector efficiencies, geometric factors and other information available from the calibration tables, and give measurements in 5 physical units in separate files:
(Differential) particle flux as ions cm**?2s**?1sr**?1keV**?1, (Differential) particle energy flux in keVcm**?2s**?1sr**?1keV**?1, particle phase space density in ions s**3 km**? 6, corrected-for-efficiency particle count rate as ions s**? 1, and raw particle counts in number of ions per counter bin. These Level 3 archival files are constructed by joining files from similar telemetry data products (same ion species, different angular, energy or time resolution). They are organized as a function of the instrument (HIA or CODIF), the operational mode (magnetospheric, solar wind, or RPA), the instrument sensitivity side (High Sensity or Low Sensity), and the 4 ion species of H+, He+, He++, and O+ with energies from ~25eV/e to 40 keV/e and with medium angular resolution of 22.5 deg (for CODIF only).
Two data processing software packages are available from CAA: the CIS_3D_MOM written in C to read the CIS Level 3 files, and another software written in IDL to read Level 1 data and calibrations files. The second software can read, in addition to CIS data, generic CDF and CEF data files for correlation studies.
The CIS data archive at CAA also includes experiment documentation, graphical products for browsing through the data, and data caveats.
For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

The Cluster Ion Spectrometry (CIS) data products include three-dimensional ion distributions (about 0-40 keV/e) in 4-s spacecraft spin resolution and mass-per-charge composition distribution that are measured by the Hot Ion Analyzer (HIA) and Composition Distribution Function (CODIF) analyzer on board the Cluster II Salsa spacecraft. Data products consist of processed raw data (Level 1 data), moments of the distribution functions (Level 2 data), and calibrated high-resolution data in a variety of physical units (Level 3 data). Furthermore, the calibration files and high-level processing software are also available.
CIS Level 1 data are decommutated, decompressed and time-tagged telemetry data in raw instrument units.
CIS Level 2 data are moments of the particle functions: ion density, velocity in the GSE reference frame, and temperature in parallel and perpendicular components (obtained by diagnolizing the pressure tensor). For CODIF, which has a higher upper energy limit than HIA, the pressure is also supplied in addition. They correspond to the Prime Parameters from the Cluster Science Data System: onboard calculated moments, then reprocessed on ground (total efficiency calibration adjustments, coordinate transformations etc.). Onboard calculated moments provide 1-spin time resolution, and are calculated from the full angular and energy resolution 3-D ion distributions.
In addition to the onboard calculated moments, CIS Level 2 data include also CODIF moments calculated on the ground from the 3-D ion distributions. These provide better calibration adjustments (per anode efficiency) and are thus more accurate, but have a reduced time and energy resolution. HIA on the ground calculated moments are not supplied, because the same anode calibrations would be used as for the onboard calculated ones, but with a degraded time, energy and angular resolution (no added value). A software package is available for download at the CAA web site, allowing the user to interactively calculate partial (or total) moments of the ion distributions, for selected energy and solid angle ranges: CODIF (all 4 ion species) and HIA data.
CIS Level 3 data are processed high-resolution 3-D ion distributions. They are produced by correcting the Level 1 data for detector efficiencies, geometric factors and other information available from the calibration tables, and give measurements in 5 physical units in separate files:
(Differential) particle flux as ions cm**?2s**?1sr**?1keV**?1, (Differential) particle energy flux in keVcm**?2s**?1sr**?1keV**?1, particle phase space density in ions s**3 km**? 6, corrected-for-efficiency particle count rate as ions s**? 1, and raw particle counts in number of ions per counter bin. These Level 3 archival files are constructed by joining files from similar telemetry data products (same ion species, different angular, energy or time resolution). They are organized as a function of the instrument (HIA or CODIF), the operational mode (magnetospheric, solar wind, or RPA), the instrument sensitivity side (High Sensity or Low Sensity), and the 4 ion species of H+, He+, He++, and O+ with energies from ~25eV/e to 40 keV/e and with medium angular resolution of 22.5 deg (for CODIF only).
Two data processing software packages are available from CAA: the CIS_3D_MOM written in C to read the CIS Level 3 files, and another software written in IDL to read Level 1 data and calibrations files. The second software can read, in addition to CIS data, generic CDF and CEF data files for correlation studies.
The CIS data archive at CAA also includes experiment documentation, graphical products for browsing through the data, and data caveats.
For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

This instrument never worked and there is no data. This instrument (CIS: Cluster Ion Spectrometry) on the other spacecraft is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

The Cluster Ion Spectrometry (CIS) data products include three-dimensional ion distributions (about 0-40 keV/e) in 4-s spacecraft spin resolution and mass-per-charge composition distribution that are measured by the Hot Ion Analyzer (HIA) and Composition Distribution Function (CODIF) analyzer on board the Cluster II Samba spacecraft. Data products consist of processed raw data (Level 1 data), moments of the distribution functions (Level 2 data), and calibrated high-resolution data in a variety of physical units (Level 3 data). Furthermore, the calibration files and high-level processing software are also available.
CIS Level 1 data are decommutated, decompressed and time-tagged telemetry data in raw instrument units.
CIS Level 2 data are moments of the particle functions: ion density, velocity in the GSE reference frame, and temperature in parallel and perpendicular components (obtained by diagnolizing the pressure tensor). For CODIF, which has a higher upper energy limit than HIA, the pressure is also supplied in addition. They correspond to the Prime Parameters from the Cluster Science Data System: onboard calculated moments, then reprocessed on ground (total efficiency calibration adjustments, coordinate transformations etc.). Onboard calculated moments provide 1-spin time resolution, and are calculated from the full angular and energy resolution 3-D ion distributions.
In addition to the onboard calculated moments, CIS Level 2 data include also CODIF moments calculated on the ground from the 3-D ion distributions. These provide better calibration adjustments (per anode efficiency) and are thus more accurate, but have a reduced time and energy resolution. HIA on the ground calculated moments are not supplied, because the same anode calibrations would be used as for the onboard calculated ones, but with a degraded time, energy and angular resolution (no added value). A software package is available for download at the CAA web site, allowing the user to interactively calculate partial (or total) moments of the ion distributions, for selected energy and solid angle ranges: CODIF (all 4 ion species) and HIA data.
CIS Level 3 data are processed high-resolution 3-D ion distributions. They are produced by correcting the Level 1 data for detector efficiencies, geometric factors and other information available from the calibration tables, and give measurements in 5 physical units in separate files:
(Differential) particle flux as ions cm**?2s**?1sr**?1keV**?1, (Differential) particle energy flux in keVcm**?2s**?1sr**?1keV**?1, particle phase space density in ions s**3 km**? 6, corrected-for-efficiency particle count rate as ions s**? 1, and raw particle counts in number of ions per counter bin. These Level 3 archival files are constructed by joining files from similar telemetry data products (same ion species, different angular, energy or time resolution). They are organized as a function of the instrument (HIA or CODIF), the operational mode (magnetospheric, solar wind, or RPA), the instrument sensitivity side (High Sensity or Low Sensity), and the 4 ion species of H+, He+, He++, and O+ with energies from ~25eV/e to 40 keV/e and with medium angular resolution of 22.5 deg (for CODIF only).
Two data processing software packages are available from CAA: the CIS_3D_MOM written in C to read the CIS Level 3 files, and another software written in IDL to read Level 1 data and calibrations files. The second software can read, in addition to CIS data, generic CDF and CEF data files for correlation studies.
The CIS data archive at CAA also includes experiment documentation, graphical products for browsing through the data, and data caveats.
For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

The Cluster Ion Spectrometry (CIS) data products include three-dimensional ion distributions (about 0-40 keV/e) in 4-s spacecraft spin resolution and mass-per-charge composition distribution that are measured by the Hot Ion Analyzer (HIA) and Composition Distribution Function (CODIF) analyzer on board the Cluster II Tango spacecraft. Data products consist of processed raw data (Level 1 data), moments of the distribution functions (Level 2 data), and calibrated high-resolution data in a variety of physical units (Level 3 data). Furthermore, the calibration files and high-level processing software are also available.
CIS Level 1 data are decommutated, decompressed and time-tagged telemetry data in raw instrument units.
CIS Level 2 data are moments of the particle functions: ion density, velocity in the GSE reference frame, and temperature in parallel and perpendicular components (obtained by diagnolizing the pressure tensor). For CODIF, which has a higher upper energy limit than HIA, the pressure is also supplied in addition. They correspond to the Prime Parameters from the Cluster Science Data System: onboard calculated moments, then reprocessed on ground (total efficiency calibration adjustments, coordinate transformations etc.). Onboard calculated moments provide 1-spin time resolution, and are calculated from the full angular and energy resolution 3-D ion distributions.
In addition to the onboard calculated moments, CIS Level 2 data include also CODIF moments calculated on the ground from the 3-D ion distributions. These provide better calibration adjustments (per anode efficiency) and are thus more accurate, but have a reduced time and energy resolution. HIA on the ground calculated moments are not supplied, because the same anode calibrations would be used as for the onboard calculated ones, but with a degraded time, energy and angular resolution (no added value). A software package is available for download at the CAA web site, allowing the user to interactively calculate partial (or total) moments of the ion distributions, for selected energy and solid angle ranges: CODIF (all 4 ion species) and HIA data.
CIS Level 3 data are processed high-resolution 3-D ion distributions. They are produced by correcting the Level 1 data for detector efficiencies, geometric factors and other information available from the calibration tables, and give measurements in 5 physical units in separate files:
(Differential) particle flux as ions cm**?2s**?1sr**?1keV**?1, (Differential) particle energy flux in keVcm**?2s**?1sr**?1keV**?1, particle phase space density in ions s**3 km**? 6, corrected-for-efficiency particle count rate as ions s**? 1, and raw particle counts in number of ions per counter bin. These Level 3 archival files are constructed by joining files from similar telemetry data products (same ion species, different angular, energy or time resolution). They are organized as a function of the instrument (HIA or CODIF), the operational mode (magnetospheric, solar wind, or RPA), the instrument sensitivity side (High Sensity or Low Sensity), and the 4 ion species of H+, He+, He++, and O+ with energies from ~25eV/e to 40 keV/e and with medium angular resolution of 22.5 deg (for CODIF only).
Two data processing software packages are available from CAA: the CIS_3D_MOM written in C to read the CIS Level 3 files, and another software written in IDL to read Level 1 data and calibrations files. The second software can read, in addition to CIS data, generic CDF and CEF data files for correlation studies.
The CIS data archive at CAA also includes experiment documentation, graphical products for browsing through the data, and data caveats.
For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

The data set provides the 5-second (spin-averaged) FAST survey data from the Time of flight Energy Angle Mass Spectrograph (TEAMS) in CDF format. The data set includes H+, O+, and He+ differential energy fluxes. Pitch-angle-averaged fluxes are provided for 48 energies (1eV-12keV). Energy-averaged fluxes are provided for 16 pitch angles (0-360 deg) for the energy range 0.01-1keV and >1keV. Each angle segment contains 2 (4) samples at each energy in the 32 (64) sweep/spin mode. The full angular range is covered in half a spin but the actual time resolution of the survey data product depends upon the telemetry mode. In the highest TM rate modes H+ and O+ survey data read out every half spin. In lowest TM rate mode these data are accumulated for 4 spins. The minimum accumulation time included in the CDF is 1 spin, so if the actual accumulation time is a half spin, two data points are averaged. Otherwise, the full resolution is included. In every mode He+ and He++ are accumulated twice as long as H+ and O+. To force the H+, O+, and He+ to have an equal number of data points when H+ and O+ have twice the time resolution, each He+ data point is written twice consecutively in the file. Orbit parameters are also included in this data set.

This quick-look data pool data set contains selected physical parameters computed centrally for each instrument at resolutions between one and five minutes, using quick-look, PI-provided algorithms. It was created in binary IBM 360 representation with unblocked, 3240-byte records. The first record of each file is a data pool file label containing satellite ID number; year, day of year, and seconds of day for the start and end of file; spacecraft clock; telemetry group number; minimum and maximum value of spin period found in this file; shadow times; and bit rate. The label record is followed by a number of data records containing day of year and seconds of day; s/c clock; bit rate; housekeeping and engineering items; spin period average; satellite position vector in GSE coordinates; and outputs of the investigators' quick-look data-processing algorithms for selected parameters from ten of the onboard experiments. The fast plasma data (Gosling/LANL) include four-level electron spectra, ion pseudondensities, average energies, and solar wind peak speeds and pseudodensities, at 5-minute resolution. The hot plasma (Frank, U. Iowa) algorithm outputs include proton densities, 10 keV electron fluxes, and energy range indicators, at 5-minute resolution. The fluxgate magnetometer data (Russell, UCLA) include 25 hourly parameters, plus the components of the magnetic field in spacecraft coordinates, at 1-minute resolution. The low-energy cosmic ray data (Hovestadt, MPI) include count rates of protons in three energy intervals between 0.17 and 20 MeV, plus those of alpha particles from 0.12 to 0.25 MeV and of Z>2 particles above 0.1 MeV, at 15-second resolution. The quasi-static electric field (Mozer, UCB) algorithm outputs indicate whether the experiment's electron guns were on or off during each 64-second interval. The plasma wave data (Gurnett, U. Iowa) include instantaneous samples from the 562 Hz filter channels of the electron and magnetic spectrum analysers, at 5-minute resolution. The plasma density data (Harvey, CESR) include indicators of the activity of the sounder and the propagation transmitters during each 64-second period. The energetic electron and proton algorithm outputs (Williams, APL) include both electron and proton differential fluxes in the 32 to 50 keV and the 80 to 126 keV energy ranges. These fluxes are taken in or near the spin-normal (nominally ecliptic) plane, at 5-minute resolution. The electron and proton experiment (K.Anderson, UCB) algorithm outputs include both electron and proton fluxes in the energy range 8 to 200 keV, at 5-minute resolution. The ion composition data (Sharp, Lockheed) include the cold plasma density and flags indicating the presence of high ion temperatures and bulk flow in the plasma, at 5-minute resolution. The Pool Tape Documentation (GSFC document X-692-77-129) (B29494 in NSSDC's Publications database) includes brief descriptions of the instruments, sometimes quite detailed, and also descriptions of the quick-look algorithms, also sometimes quite detailed.

This ASCII file contains values and their uncertainties
for 25 abundance ratios of various pairs of chemical elements. The ratios
are based on 1978-1981 observations of ~50-500 MeV/n cosmic rays by the
U. Chicago cosmic ray experiment on ISEE 3. Each of the ratios is linked
in the ASCII file to the publication where its derivation is discussed.

This data product consists of a single ASCII file
containing values and their uncertainties for 32 abundance ratios of
various pairs of isotopes of 13 chemical elements (C, O, Ne, Mg, Al,
Si, Ti, V, Cr, Mn, Fe, Co, Ni). Between this data product and a
companion catalog with isotopic fractions, isotopic composition
information is given for 21 chemical elements. The ratios are based
on 1978-1981 observations of ~50-500 MeV/n cosmic rays by the U.
Chicago cosmic ray experiment on ISEE 3. Each of the ratios is
linked in the ASCII file to the publication where its derivation is
discussed.

This data product consists of a single ASCII file
containing values and their uncertainties for isotopic fractions of 56
specific isotopes relative to isotope-integrated elemental abundances,
for 15 elements (Be, B, N, S, Cl, Ar, K, Ca, Ti, V, Cr, Mn, Fe, Co, Ni).
Between this data product and a companion product with isotopic abundance
ratios, isotopic composition information is given for 21 chemical elements.
The fractions are based on 1978-1981 observations of ~50-500 MeV/n cosmic
rays by the U. Chicago cosmic ray experiment on ISEE 3. Each of the ratios
is linked in the ASCII file to the publication where its derivation is
discussed.

This set of plasma data came from the ISIS 2 (International Satellites for Ionospheric Studies) ion-mass spectrometer experiment. Ion densities of various ion species are available for the lower range (1-8 atomic mass units, H+, D+, He+, N++, O++) and the upper range (8-64 atomic mass units, O++, N+, O+, 18+, N2+, NO+, O2+). Also included in the data set are spacecraft position data, geomagnetic field intensity, F107 flux (daily solar radio flux), Kp indices, and Dst indices.

Mass resolved ion energy angle spectra covering nearly the full 4pi solid angle and the energy range 15 eV/q to 33 eV/q.
H+, O+, He+ and He++ number fluxes and statistical uncertainties processed by the TIMAS science team. Data acquired with various angular and energy resolutions are combined here. Data Quality and other indicators are provided to allow selection of high resolution data (PA_status(ion)=0 and Energy_status(ion)=0 ) and High Quality data (Quality=0). See caveats for the following variables for more detailed information: Quality, PA_status, Energy_status Bcr, Fec, Even_odd, Energy_Range_ID and Spins.
Reference:E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995.
Version 0: December, 1997
Version 1: July, 1998
Version 2: December, 2000
Algorithm improved to more accurately subtract backgrounds arising from spill over from H+ into He++ channel and other sources. Fill data are now inserted for limited energy and pitch angle ranges for Flux_H Flux_O Flux_He_1 and Flux_He_2 variables. The meanging of values of the of Quality variable was slightly modified.
Version 3: June, 2002
Algorithm for V_02 had an error that resulted in under estimation of fluxes in high count regions, i.e. the cusp/cleft and radiation belts. V_03 corrects this error and has been expanded to include calculation of fluxes obtained after December 8, 1998, when TIMAS had a damaging high voltage breakdown that resulted in reduced sensitivity.

Mass spectra count rates for survey purposes only from the POLAR TIMAS instrument. The mass spectral data product consists of 64 mass steps covering the full detector range, for each of 6 large solid angles, for 8 selected energy steps. The data product is accumulated for 2, 4, 8, 16, or 32 spin (6 s) periods. Because of telemetry restrictions only selected data products were telemetered to the ground.
The 6 angular bins cover the full instrumental range and nearly 4pi steradians. Two of the look directions are centered on the spacecraft spin axis. For the first part of the mission, the spin axis was orbit normal and the pitch angles sampled in these look directions are near 90 degrees. The other 4 look directions are in the spin plane. Data are de-spun on board based on the spin rate and time of the "sun pulse". The digital data product provides the center pitch angle of each of the 6 look directions and an estimate of the variation of the pitch angle during the accumulation time.
Reference: E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995.

This data set contains ion data from the ROCSAT-1 Ionospheric Plasma and Electrodynamics Instrument (IPEI). They include: composition for H+, He+, NO+, O+ ions, total density, temperature, and velocities in two different coordinate systems, namely the non-rotating Earth-centered Inertia (ECI) Coordinate System and the rotating Earth-centered Fixed (ECF) Coordinate System.

This data set contains 17 differential fluxes of
protons (mainly), helium ions, Z.GE.6 ions, and electrons, plus one integral
flux of protons and electrons, as averaged over polar cap passes of the
SAMPEX spacecraft. A polar cap pass covers the time poleward of geomagnetic
latitude 70 deg. (Not all orbits have two polar cap passes.). For any
given species, the fluxes typically come from more than one of the sensors
(LICA, HILT, MAST, PET). Hence the inclusion of all instruments' data in
each single record. Differential fluxes are those for (mainly) protons
(Z.GE.1 channels at 5-12 and 19-27 MeV/n), helium ions (0.50-6.6, 4-9, 8-15,
9-38 MeV/n), Z.GE.6 ions (0.49-8.3, 8-42, 19.3-22.8, 22.8-31.0, 31.0-51.7,
41-220, 51.7-76.2, 76.2-113, 113-156 MeV/n), and electrons (1.5-6.0 MeV
from PET only). One LICA channel measured integral fluxes of ions .GT. 0.8 MeV/n
plus electrons .GT. 0.6 MeV). Data available for each polar cap pass are time
tags of the begin and end points of the averaging interval, the fluxes,
statistical uncertainties in the fluxes, instrument-specific flags, and a
flag indicating a north or south polar cap pass. Data are organized in two
different ways. Monthly ~500-KB ASCII files with records organized by instrument
are available from the SAMPEX Data Center at Caltech and from nssdcftp at
GSFC/SPDF, while monthly ~260 KB CDF-formatted files with records organized by
species are available from the ftp area underlying CDAWeb. The parameter level
information given below in this descriptor corresponds to the CDAWeb organization
of data. Format information for the ASCII version is given in the Information
URL of this descriptor.

This set of 30-s averaged fluxes are derived from measurements made by all 4 instruments (HILT, LICA, MAST and PET) onboard the Solar Anomalous and Magnetospheric Particle Explorer (SAMPEX). Each file covers one full day of 30-s averaged fluxes of cosmic rays from selected channels from all experiments. There are 156 variables per record, and the file size is about 4 MB. After an extensive list of ancillary data, the particle fluxes follow. (1) LICA provides fluxes of electrons and protons in the energy range of about >0.7 Mev, of (mainly) helium in the range 0.49-8.3 MeV/nucleon. (2) HILT provides fluxes of helium from two channels, 4-9 and 9-38, of Z > 5 from two channels, 8.2-42 and 41-220 MeV/n. (3) MAST provides fluxes protons (mainly) in 5-12 MeV range, of helium in 8-15, and of Z > 5 in 19.3-22.8, 22.8-31.0, 31.0-51.7, 51.7-76.2, 76.2-113, 113-156 MeV/n. (4) PET provides fluxes of electrons in the ranges 1.5-6, and 2.5-14 MeV, and of (mainly) protons in 19-27 MeV/n. All flux values are accompanied by their standard deviations and quality flags. The fluxes available in this file are from a subset of (30-s resolution) rate channels. Energy spectra are assembled by pick-and-choose across instrument boundaries; an example is the eight-element array of Z>3 fluxes that have contributions from all four instruments

THEMIS-A On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations.
Table 1: Coordinate Descriptions.
Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system.
Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system.
Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis.
Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system.

THEMIS-A: The Solid State Telescope (SST) measures the incoming intensity (flux per solid angle) of superthermal electrons and ions. The spacecraft is fitted with two units (heads), each SST unit has two pairs of opposing ion and electron sensors. Each single sensor covers an angle of 36 degrees. The units are oriented such that one pair is always centered in the rotation plane, the other oriented at a maximum angle of 54 degrees off the plane. Each pair of units are oriented opposite each other allowing both ion and electron sensors to sweep out a maximum of 92% of the sky (45x45 degree required Elevation by Azimuth FOV, 108x22 raw) . The ion and electron sensors primarily measure particles between 30-300 keV and 30-100 keV respectively with a maximum capability of 20-6000 keV and 25-1000 keV. Full distribution data is measured over 128 angles and 16 energy bins, reduced distribution uses 6 angles and 16 energy bins, and burst mode data has 64 angles in 16 energy bins. Matched and paired electron broom magnets produce quadrapole fields reducing magnetic contamination. A mechanical attenuator is used to increase the instruments dynamical range avoiding oversaturation near the plasma sheet edge.

THEMIS-B On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations.
Table 1: Coordinate Descriptions.
Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system.
Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system.
Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis.
Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system.

THEMIS-B: The Solid State Telescope (SST) measures the incoming intensity (flux per solid angle) of superthermal electrons and ions. The spacecraft is fitted with two units (heads), each SST unit has two pairs of opposing ion and electron sensors. Each single sensor covers an angle of 36 degrees. The units are oriented such that one pair is always centered in the rotation plane, the other oriented at a maximum angle of 54 degrees off the plane. Each pair of units are oriented opposite each other allowing both ion and electron sensors to sweep out a maximum of 92% of the sky (45x45 degree required Elevation by Azimuth FOV, 108x22 raw) . The ion and electron sensors primarily measure particles between 30-300 keV and 30-100 keV respectively with a maximum capability of 20-6000 keV and 25-1000 keV. Full distribution data is measured over 128 angles and 16 energy bins, reduced distribution uses 6 angles and 16 energy bins, and burst mode data has 64 angles in 16 energy bins. Matched and paired electron broom magnets produce quadrapole fields reducing magnetic contamination. A mechanical attenuator is used to increase the instruments dynamical range avoiding oversaturation near the plasma sheet edge.

THEMIS-D On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations.
Table 1: Coordinate Descriptions.
Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system.
Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system.
Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis.
Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system.